Multidimensional relativistic MHD simulations of Pulsar Wind Nebulae: dynamics and emission

Abstract

Pulsar Wind Nebulae, and the Crab nebula in particular, are the best cosmic laboratories to investigate the dynamics of magnetized relativistic outflows and particle acceleration up to PeV energies. Multidimensional MHD modeling by means of numerical simulations has been very successful at reproducing, to the very finest details, the innermost structure of these synchrotron emitting nebulae, as observed in the X-rays. Therefore, the comparison between the simulated source and observations can be used as a powerful diagnostic tool to probe the physical conditions in pulsar winds, like their composition, magnetization, and degree of anisotropy. However, in spite of the wealth of observations and of the accuracy of current MHD models, the precise mechanisms for magnetic field dissipation and for the acceleration of the non-thermal emitting particles are mysteries still puzzling theorists to date. Here we review the methodologies of the computational approach to the modeling of Pulsar Wind Nebulae, discussing the most relevant results and the recent progresses achieved in this fascinating field of high-energy astrophysics.

29 pages review, preliminary version. To appear in the book "Modelling Nebulae" edited by D. Torres for Springer, based on the invited contributions to the workshop held in Sant Cugat (Barcelona), June 14-17, 2016

References in corpus (10)

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• MPI-AMRVAC for Solar and Astrophysics
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Cited by in corpus (5)

• Gamma-ray halos around pulsars as the key to understanding cosmic ray transport in the Galaxy
• A Laminar Model for the Magnetic Field Structure in Bow-Shock Pulsar Wind Nebulae
• Escape of High Energy Particles from Bow-Shock Pulsar Wind Nebulae
• PeV proton acceleration in Gamma-ray Binaries
• New estimate for the contribution of the Geminga pulsar to the positron excess